Black Hole Formation and Fallback during the Supernova Explosion of a 40 M Star

Conrad Chan, Bernhard Müller, Alexander Heger, Rüdiger Pakmor, Volker Springel

Research output: Contribution to journalArticleResearchpeer-review

15 Citations (Scopus)

Abstract

Fallback in core-collapse supernovae is considered a major ingredient for explaining abundance anomalies in metal-poor stars and the natal kicks and spins of black holes (BHs). We present a first 3D simulation of BH formation and fallback in an "aborted" neutrino-driven explosion of a 40 solar mass zero-metallicity progenitor from collapse to shock breakout. We follow the phase up to BH formation using the relativistic CoCoNuT-FMT code. For the subsequent evolution to shock breakout we apply the moving-mesh code Arepo to core-collapse supernovae for the first time. Our simulation shows that despite early BH formation, neutrino-heated bubbles can survive for tens of seconds before being accreted, leaving them sufficient time to transfer part of their energy to sustain the shock wave as is propagates through the envelope. Although the initial net energy (∼2 Bethe) of the neutrino-heated ejecta barely equals the binding energy of the envelope, 11 M of hydrogen are still expelled with an energy of 0.23 Bethe. We find no significant mixing and only a modest BH kick and spin, but speculate that stronger effects could occur for slightly more energetic explosions or progenitors with less tightly bound envelopes.

Original languageEnglish
Article numberL19
Number of pages6
JournalAstrophysical Journal Letters
Volume852
Issue number1
DOIs
Publication statusPublished - 1 Jan 2018

Keywords

  • methods: numerical
  • stars: black holes
  • stars: massive
  • supernovae: general

Cite this

@article{4ae6b700a3774c3facc507d43d07f7e1,
title = "Black Hole Formation and Fallback during the Supernova Explosion of a 40 M⊙ Star",
abstract = "Fallback in core-collapse supernovae is considered a major ingredient for explaining abundance anomalies in metal-poor stars and the natal kicks and spins of black holes (BHs). We present a first 3D simulation of BH formation and fallback in an {"}aborted{"} neutrino-driven explosion of a 40 solar mass zero-metallicity progenitor from collapse to shock breakout. We follow the phase up to BH formation using the relativistic CoCoNuT-FMT code. For the subsequent evolution to shock breakout we apply the moving-mesh code Arepo to core-collapse supernovae for the first time. Our simulation shows that despite early BH formation, neutrino-heated bubbles can survive for tens of seconds before being accreted, leaving them sufficient time to transfer part of their energy to sustain the shock wave as is propagates through the envelope. Although the initial net energy (∼2 Bethe) of the neutrino-heated ejecta barely equals the binding energy of the envelope, 11 M⊙ of hydrogen are still expelled with an energy of 0.23 Bethe. We find no significant mixing and only a modest BH kick and spin, but speculate that stronger effects could occur for slightly more energetic explosions or progenitors with less tightly bound envelopes.",
keywords = "methods: numerical, stars: black holes, stars: massive, supernovae: general",
author = "Conrad Chan and Bernhard M{\"u}ller and Alexander Heger and R{\"u}diger Pakmor and Volker Springel",
year = "2018",
month = "1",
day = "1",
doi = "10.3847/2041-8213/aaa28c",
language = "English",
volume = "852",
journal = "The Astrophysical Journal Letters",
issn = "2041-8205",
publisher = "American Astronomical Society",
number = "1",

}

Black Hole Formation and Fallback during the Supernova Explosion of a 40 M Star. / Chan, Conrad; Müller, Bernhard; Heger, Alexander; Pakmor, Rüdiger; Springel, Volker.

In: Astrophysical Journal Letters, Vol. 852, No. 1, L19, 01.01.2018.

Research output: Contribution to journalArticleResearchpeer-review

TY - JOUR

T1 - Black Hole Formation and Fallback during the Supernova Explosion of a 40 M⊙ Star

AU - Chan, Conrad

AU - Müller, Bernhard

AU - Heger, Alexander

AU - Pakmor, Rüdiger

AU - Springel, Volker

PY - 2018/1/1

Y1 - 2018/1/1

N2 - Fallback in core-collapse supernovae is considered a major ingredient for explaining abundance anomalies in metal-poor stars and the natal kicks and spins of black holes (BHs). We present a first 3D simulation of BH formation and fallback in an "aborted" neutrino-driven explosion of a 40 solar mass zero-metallicity progenitor from collapse to shock breakout. We follow the phase up to BH formation using the relativistic CoCoNuT-FMT code. For the subsequent evolution to shock breakout we apply the moving-mesh code Arepo to core-collapse supernovae for the first time. Our simulation shows that despite early BH formation, neutrino-heated bubbles can survive for tens of seconds before being accreted, leaving them sufficient time to transfer part of their energy to sustain the shock wave as is propagates through the envelope. Although the initial net energy (∼2 Bethe) of the neutrino-heated ejecta barely equals the binding energy of the envelope, 11 M⊙ of hydrogen are still expelled with an energy of 0.23 Bethe. We find no significant mixing and only a modest BH kick and spin, but speculate that stronger effects could occur for slightly more energetic explosions or progenitors with less tightly bound envelopes.

AB - Fallback in core-collapse supernovae is considered a major ingredient for explaining abundance anomalies in metal-poor stars and the natal kicks and spins of black holes (BHs). We present a first 3D simulation of BH formation and fallback in an "aborted" neutrino-driven explosion of a 40 solar mass zero-metallicity progenitor from collapse to shock breakout. We follow the phase up to BH formation using the relativistic CoCoNuT-FMT code. For the subsequent evolution to shock breakout we apply the moving-mesh code Arepo to core-collapse supernovae for the first time. Our simulation shows that despite early BH formation, neutrino-heated bubbles can survive for tens of seconds before being accreted, leaving them sufficient time to transfer part of their energy to sustain the shock wave as is propagates through the envelope. Although the initial net energy (∼2 Bethe) of the neutrino-heated ejecta barely equals the binding energy of the envelope, 11 M⊙ of hydrogen are still expelled with an energy of 0.23 Bethe. We find no significant mixing and only a modest BH kick and spin, but speculate that stronger effects could occur for slightly more energetic explosions or progenitors with less tightly bound envelopes.

KW - methods: numerical

KW - stars: black holes

KW - stars: massive

KW - supernovae: general

UR - http://www.scopus.com/inward/record.url?scp=85040346071&partnerID=8YFLogxK

U2 - 10.3847/2041-8213/aaa28c

DO - 10.3847/2041-8213/aaa28c

M3 - Article

VL - 852

JO - The Astrophysical Journal Letters

JF - The Astrophysical Journal Letters

SN - 2041-8205

IS - 1

M1 - L19

ER -